2017 Solar Eclipse Project Outline Project Development: Keith Morin KG7QCK Updated: March 14, 2015 V3.0

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1 2017 Solar Eclipse Project Outline Project Development: Keith Morin KG7QCK Updated: March 14, 20 V3.0 I. Project Name The Great Radio Atmospheric Propagation Experiment (GRAPE) II. Scope of the Eclipse Experiment The scope of this experiment is to document the global transmission and reception characteristics of radio spectrum signals before, during, and after (BDA) the US total solar eclipse event of August 21, III. Site Function Organization The primary ground based data site considerations should be divided into three groups. Group A: Transmission Effects The global BDA effects will include any observed changes in SWR, ERP, or PEP to the transmitting station, especially those stations located within the path of totality. Group B: Reception Effects The global BDA effects will include any changes in Signal Strength or SNR to known sources such as radio beacons or NIST WWV broadcast signals at the receiving station, especially those stations located within the path of totality. Group C: Zone of Totality The data of BDA effects to point to point communications between stations located within the path of totality will be of special interest. The zone is approximately 2,500 by 73 miles in area. IV. Antenna Configuration It would be of special interest to characterize the performance of the type of antenna the individual station is using during the experiment. Such considerations will be vertical/horizontal, long wire (end or center tap), satellite dish, or circular polarizing techniques Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 1 of

2 V. Communication Bands The primary frequency bands for this project should be: All 16 US Primary Amateur Radio Bands All known radio beacon Bands VLF Radio Astronomy Bands (20 to 30 KHZ) ULF Radio Spectrum DC to 20 HZ Any Satellite Bands for voice, video, data Global Intermagnet Network The secondary frequency bands for this project will be: Local Commercial Digital Television Local Commercial AM Radio Local Commercial FM Radio Satellite Radio Satellite Television VI. Point to Point Communication Pathways Each station (TX/RX) or RX Only (DXers) will designate their selected contact during the event as: Stations located North of the Path of Totality within the Contiguous US Stations where either TX or RX occur within 25 miles of the center of the Path of Totality Stations where both TX/RX occur within 25 miles of the center of the Path of Totality Stations located South of the Path of Totality within the Contiguous US Stations located by Latitude/Longitude outside the Continental United States VII. Communication Modes AM FM USB LSB CW Video Data Receive Only Manual or Automatic Modes Automatic Modes Disabled 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 2 of

VIII. Project Satellite and Ground Based Data Sources US Geological Survey Ground Based Geomagnetic Monitoring Network The USGS maintain 14 geomagnetic automated stations.

3 VIII. Project Satellite and Ground Based Data Sources US Geological Survey Ground Based Geomagnetic Monitoring Network The USGS maintain 14 geomagnetic automated stations. Each station provides 4 measurements each. If the station locations are plotted with the path of Totality, most of these stations should detect ionospheric changes that may be used in the propagation final report. There would effectively be 56 channels of 1 minute data. DSCOVR Satellite Observatory- Launch February 8, 20. ACE Satellite Observatory- the ACE Satellite provides the monitoring of solar wind, electrons, protons, and other data that may contribute to ionospheric conditions. The data stream consists of 25 channels of data. GOES 13 and Satellite Observatory- the GOES Spacecraft provides 25 channels of 1 minute data. Solar Dynamics Observatory- the SDO provides 19 channels of solar images and 3 channels of EVE 1 minute Diode data. Combined this provides approximately 6 channels of US data to be used with ground based observations. Global Intermagnet Network can provide additional data from global ground based stations. Other Sources: Internet Wireless (IRLP) Sources Data Communications from Ocean Stationary Vessels or Buoys 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 3 of

4 IX. Event Timeline Start: 1400 UTC 08/21/2017 this will provide about 2 hours of baseline data. Event UTC State Near City (C1) 1604 Oregon Lincoln City (C2) 1717 Oregon Lincoln City (C2) 1725 Oregon Ontario (C2) 1725 Idaho Welser (C2) 1735 Idaho Driggs (C2) 1735 Wyoming Wilson (C2) 1748 Wyoming Torrington (C2) 1748 Nebraska Mitchell (C2) 1805 Nebraska Falls City (C2) 1805 Kansas Marysville (C2) 1808 Kansas Leavenworth (C2) 1808 Missouri St. Joseph (C2) 1820 Missouri Arnold (C2) 1820 Illinois Waterloo (C2) 1821 Illinois Lat: Lon: <161 sec (Longest Duration)> (C2) 1823 Illinois Harrisburg (C2) 1823 Kentucky Paducah (C2) 1825 Kentucky Lat: Lon: <Greatest Totality> (C2) 1827 Kentucky Bowling Green (C2) 1827 Tennessee Clarksville (C2) 1835 Tennessee Madisonville (C2) 1835 North Carolina Milltown (C2) 1836 North Carolina Brevard (C2) 1836 Georgia Blairsville (C2) 1837 Georgia Elberton (C2) 1837 South Carolina Easley (C2) 1847 South Carolina Georgetown (C3) 1849 South Carolina Georgetown (C4) 2010 South Carolina Georgetown End: 0000 UTC 08/22/2017 this will provide 10 hours of eclipse data. Notes: UTC Times to Minute (approx) (C1) Start Partial Eclipse (C2) Start Total Eclipse (C3) End Total Eclipse (C4) End Partial Eclipse BDA Data sampling intervals will be adjusted to site location by longitude and latitude. The circumstances of event totality at each location will be provided by the US Naval Observatory Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 4 of

5 X. Measurements Most if not all observation measurements will not be calibrated or measured to any degree of scientific accuracy. However, the observations can reflect a great deal about signal changes as expressed in a percentage of gain or loss over a period of time before, during and after the event. The project time base will utilize the NIST WWV clock signal for time and signal strength coordination which may reflect small signal discrepancies dispersed over such a large area. The Boulder Colorado WWV transmitter location will experience about 90% eclipse totality during the event. This signal is a great source for DXers (receive only) to use during the eclipse event for signal amplitude changes. XI. Global Project Participation Global partners who wish to participate in this project might include: ARRL The United Kingdom OfCom- Rutherford Appleton Laboratory Amateur Radio Society of Great Britain (GB2RS) Australia The Wireless Institute of Australia National Research Council of Canada Office of Communications Research Radio Amateurs of Canada XII. Citizen Participation Participants will be able to support the project in several different ways. The final list will be available in the near future as project planning continues. Ham operators with field experience and equipment will be of special interest in the totality region. Some areas are very remote with limited access. These locations also have little outside interference from manmade electrical or RF sources. The eclipse occurs during the late summer with many planning the start of the school year or ending their summer vacations. Planning ahead of time will be important, as many groups are planning events for the eclipse time period in the same eclipse totality region. Equipment Each participant will provide his/her own equipment of fixed, mobile, or field configuration. Important Documentation Event Registration Information to obtain Site ID Number Running Time Log of observations Submit Time Log Data with site final event configuration and location after the event 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 5 of

6 XIII. Participant Registration and Recognition Participant Registration Registration for this event will be scheduled to begin January 1, 2017 Registration for this event will be scheduled to close June 1, 2017 Participant Information Week of June 30, 2017 Participant Training Day Saturday, July, 2017 Participant Tabletop Exercise Day Saturday, July 22, 2017 Participant Special Considerations Day Saturday, July 29, 2017 Participant Final Instructions Day Saturday, August 5, 2017 Participants in this project should be recognized for their contributions and efforts. Some suggestions will be: Project Patch Project Hat, T-shirt, or other apparel Project Poster or decal Project Final Report Copy Citation in a any scientific paper that is produced 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 6 of

7 XIV. Proposed Project Milestones 20 February 28-Complete Initial Draft-Project Outline February 28-Create Project Name and Logo Create Project Milestones 2016 Create Participant Documentation Package 2017 Registration for this event will be scheduled to begin January 1, 2017 Event Tabletop Exercise Registration for this event will be scheduled to close June 1, 2017 Participant Information Week of June 30, 2017 Participant Training Day Saturday, July, 2017 Participant Tabletop Exercise Day Saturday, July 22, 2017 Participant Special Considerations Day Saturday, July 29, 2017 Participant Final Instructions Day Saturday, August 5, 2017 Solar Eclipse Event Begins August 21, 2017 Participants Submit Data Begin Data Evaluation 2018 Complete Project Final Report 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 7 of

8 XV. References and Resources NASA 2017 Eclipse Website: USNO Eclipse Portal: Space Weather Prediction Center Website: USGS Geomagnetic Observatory Website: Intermagnet Website: Solar Dynamics Observatory Website: ACE Satellite Website: GOES Website: <moved to Space Weather Prediction Center> CATE Website: NOAO CATE Website: OfCom RCRU Rutherford Appleton 1999 UK Eclipse Final Report Interactive Google Map of 2017 Eclipse Webpage: 89&Zoom=4&Map=G_NORMAL_MAP Eclipse 2017.org Website: Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 8 of

9 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 9 of

10 "Eclipse Predictions by Fred Espenak, NASA's GSFC" 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 10 of

11 "Eclipse Predictions by Fred Espenak, NASA's GSFC 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 11 of

12 Sample Graphics 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 12 of

The moon eclipses the GOES SXI Imager on Satellite on 10-23-14.

13 The moon eclipses the GOES SXI Imager on Satellite on Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 13 of

14 Example of a raw image. The moon eclipses the satellite. (SDO Image 2254 UTC) 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page 14 of

15 NASA GSFC Animated gif of Eclipse US Naval Observatory Animated gif of Eclipse 2017 Solar Eclipse Project V2.0 3/14/20 12:21:08 PM Page of

Eclipse 20 RADIO SOCIETY OF GREAT BRITAIN RADIO PROPAGATION EXPERIMENT ON MARCH 20 How you can take part in a scientific experiment On Friday March 20 a partial solar eclipse will be visible from the

This is a great opportunity to try a simple experiment to see how the sun s ultra violet output affects our ionosphere, which alters how some radio waves are propagated around the world.

16 Eclipse 20 RADIO SOCIETY OF GREAT BRITAIN RADIO PROPAGATION EXPERIMENT ON MARCH 20 How you can take part in a scientific experiment On Friday March 20 a partial solar eclipse will be visible from the UK. The path of totality will pass north of the UK, but we will experience up to 89% totality (depending upon where you live). This is a great opportunity to try a simple experiment to see how the sun s ultra violet output affects our ionosphere, which alters how some radio waves are propagated around the world. By using just a portable medium wave radio you may be able to see this effect for yourself. Want to take part? Read on! The sun s effect on the ionosphere The sun s ultra- violet (UV) output has a profound effect on the upper reaches of the earth s atmosphere. At altitudes higher than about km the sun s UV energy ionises the atoms and molecules of the rarified gases that make up what we call the ionosphere. The high- energy UV photons knock electrons out of their atoms, predominantly nitrogen and oxygen, leaving charged particles or ions. These ions can be found in a number of distinct regions or layers and have the ability to reflect or absorb radio waves, depending on the amount of ionisation and the frequency of the wave. The lowest region is called the D layer and is very effective at absorbing medium wave transmissions at about 1 MHz during the day, when it is exposed to the sun. At night the ions and electrons recombine and the layer vanishes. If we listen for a medium wave (MW) radio station more than miles away during the day we may not hear it it is too far away for its ground wave signal to reach us, and any sky wave signal is absorbed by the D layer. But at night its sky wave signals are not absorbed as there is no D layer. They are free to be reflected back to earth from the higher E layer, which is weaker than it is during the day, but still exists. This is why you can hear distant medium wave stations on a radio at night time, but you can t hear them during the day. But what about during a partial solar eclipse? On the morning of Friday March the D layer above the UK may not be as strong, and you may be able to hear distant stations that would otherwise be inaudible. To be honest, we don t really know just how the partial eclipse will affect MW radio propagation, which is why we need your help. With a simple portable medium wave radio you can help RSGB by conducting an experiment at the time of the eclipse. The information will also be shared with the Rutherford Appleton Laboratory. Go to page two to find out how you can take part. Find out more about amateur radio at What is a solar eclipse? A partial solar ecl i p s e. I m age : Wi k i m e d i a. A solar eclipse occurs when the moon moves between the earth and the sun, casting a shadow on the earth s surface. With a partial solar eclipse it looks like a bite has been taken out of the sun as the moon obscures part of the sun s disk. Note: you should never look directly at the sun without suitable eye protection. A partial eclipse is observed from Earth when it is in the Moon s outer shadow or penumbra. This is what we will experience in the UK on Friday March the path of totality will pass north of the UK, over the Faroe Islands. You can find out more at How an eclipse occurs. Image: Wikimedia.

The experiment - what you need to do The aim of the experiment To see how a partial solar eclipse might affect long distance medium wave (MW) reception in the UK.

17 The experiment - what you need to do The aim of the experiment To see how a partial solar eclipse might affect long distance medium wave (MW) reception in the UK. The equipment You will need a portable medium wave radio, or car radio, with a digital frequency display. You then need to find a suitable medium wave station for the experiment. It has to be a station that is far enough away that you cannot normally hear it during the day, but is audible at night. Ideally, you need to pick one at least miles from your location. Here is a list of suggested stations: BBC Radio Wales 882 khz (transmitter: Washford Somerset). BBC Radio Scotland 810 khz (transmitters: Burghead/Westerglen). Smooth Radio 1332 khz (transmitter: Peterborough). Nostalgia (Netherlands) 747 khz (transmitter: Zeewolde). We suggest spending a day or two in advance of the eclipse seeing if you can hear one of the stations at night, but not during the day. As a tip, try to choose the station furthest away from you. You might have to rotate the radio for maximum signal strength. On the day Friday March 20 The partial eclipse starts in the Midlands at about 08:25 GMT and ends at 10:41 GMT. Maximum eclipse will be at about 09:30 GMT. The exact times will vary depending upon your location. We suggest monitoring your chosen station from about 08. to 11:30 GMT. If possible, record the audio during whole period so that you can review it later. It might be worth announcing the time on the recording at regular intervals too so that you have a reference. Or make a separate note of any effect you see and the elapsed time since you started the recording. From a scientific perspective it might be a good idea to make a similar recording of the frequency between 08: and 11:30 GMT the previous day for reference purposes. What we want to know When you have completed the Taking the experiment further If you are a radio amateur, short wave listener or have more advanced equipment you might want to take the experiment a little further. Here are some ideas: l If you have a software defined radio (SDR) you might want to note the signal strength of your chosen station in dbm every five minutes. You could then graph the results. l You could connect the audio output of your receiver to your computer sound card and use SpectrumLab or similar software to log the audio output strength every minute. This could then be graphed. Note: you must turn off the receiver s automatic gain control (AGC) to get meaningful results. l Don t forget to repeat the experiment at the same time the day before so that you can make a comparison. l If you log the same signal for all 24 hours of March 20 you could compare the received signal strength during the night and during the eclipse period and see if there is a difference. l Radio clubs could make this a project with members logging different stations. You could also monitor other signals during the period, including signals on VLF, LF, the amateur or short wave broadcast bands. For example, Iceland has two long wave stations on 189 and 207 khz. experiment, send an e- mail to the project coordinator Steve Nichols at psc.chairman@rsgb.org.uk with the following information: 1. Your name/school name. 2. Your nearest town and postcode. 3. The type of radio receiver you used. 4. The station you listened for and its frequency. 5. Then answer the questions: Were you able to hear the station at night from your location? 6. Were you able to hear the station at the begining of your test? 7. Were you able to hear the station during the eclipse period? 8. If you could, at what time was it loudest and when did it vanish? Feel free to add any other comments if you wish. The results of the experiment will be collated and appear in RadCom, the Radio Society of Great Britain's monthly journal. All participants will receive a complimentary PDF copy of the feature when it is produced. You can find out more about the RSGB at How medium wave (MF, 300 khz to 3 MHz) and short wave (SW, 3-30 MHz) radio waves can be reflected/refracted from the different layers of the ionosphere during the day and during an eclipse or at night. If you have any questions about the experiment, contact Steve Nichols G0KYA, the project coordinator at psc.chairman@rsgb.org.uk

Chapter 6 Propagation

Chapter 6 Propagation Al Penney VO1NO Objectives To become familiar with: Classification of waves wrt propagation; Factors that affect radio wave propagation; and Propagation characteristics of Amateur